2004 Denver Annual Meeting (November 710, 2004)
Paper No. 5-10
Presentation Time: 10:30 AM-10:45 AM


BURT, Donald M., Visiting Scientist, Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, TX 77058-1113 and KNAUTH, L. Paul, Geological Sciences, Arizona State Univ, Box 1404, Tempe, AZ 85287-1404, knauth@asu.edu

Images and preliminary data from Opportunity lander do not provide convincing evidence for aqueous sedimentation and later formation of diagenetic concretions. The light-colored layers are better explained by mechanical emplacement following impacts into a megaregolith holding concentrated brines and salts (Knauth and Burt, 2002; Burt and Knauth, 2003).

The Opportunity site lies among possible rampart craters and ejecta aprons usually interpreted as the result of impact into wet targets. Owing to evaporation followed by fractional crystallization during freezing of the early hydrosphere, the megaregolith over large regions must contain subsurface crystalline salts and near-eutectic brines as well as water ice. Large impacts into such material should generate ejecta sheets resembling base surge (explosion) deposits around terrestrial volcanoes, but on a far larger scale. Such deposition commonly produces finely laminated, cross-bedded, and lapilli-rich deposits almost indistinguishable from those observed at the Oppportunity site. For large impacts, vapor condensate spherules could occur as well as lapilli and accretionary lapilli. Such features provide a simple explanation for the uniformly-sized and rounded Mars "blueberries," which lack the morphologic and size distribution features of terrestrial concretions.

In this scenario, the chloride, sulfate, and bromide salts found by Opportunity were deposited mechanically along with the mainly basaltic materials, ice, and brine. Following emplacement, interactions of the fresh ejecta with the martian atmosphere over long times would allow the hygroscopic eutectic chloride and bromide salts to deliquesce and flow downwards, or be washed into the deeper regolith during ice melting to account for the vugs. Differential solubility can preferentially remove chlorides and bromides and leave sulfates. Slow atmospheric weathering could also account for oxidation of Fe in near-surface spherules and alteration of emplaced sulfides to jarosite. Features at the Opportunity site thus do provide additional evidence of an early hydrosphere on Mars, but it had already disappeared into the megaregolith when impacts produced this remarkable deposit.

2004 Denver Annual Meeting (November 710, 2004)
General Information for this Meeting
Session No. 5
Planetary Geology
Colorado Convention Center: 605
8:00 AM-12:00 PM, Sunday, 7 November 2004

Geological Society of America Abstracts with Programs, Vol. 36, No. 5, p. 21

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